NGC 3516
NGC 3516 by Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension11h 06m 47.5s[1]
Declination+72° 34′ 07″[1]
Redshift0.008836 ± 0.000023 [1]
Heliocentric radial velocity2649 ± 7 km/s[1]
Distance165 ± 50 Mly (51.5 ± 15.1 Mpc)[1]
Apparent magnitude (V)11.5[2]
Characteristics
Type(R)SB(s)0^0^ [1]
Apparent size (V)1.7′ × 1.3′[1]
Notable featuresSeyfert galaxy
Other designations
UGC 6153, MCG +12-11-009, PGC 33623[1]

NGC 3516 is a barred lenticular galaxy in the constellation of Ursa Major. NGC 3516 is located about 150 million light years away from Earth, which means, given its apparent dimensions, that NGC 3516 is approximately 100,000 light years across. It was discovered by William Herschel on April 3, 1785.[3]

Characteristics

In 1943, this galaxy was one of six nebulae listed by American astronomer Carl Keenan Seyfert that showed broad emission lines in their nuclei.[4] Members of this class of objects became known as Seyfert galaxies, and they were noted to have a higher than normal surface brightness in their nuclei. NGC 3516 is believed to host a supermassive black hole whose mass is estimated to be (4.27±1.46)×107 M☉ based on broad emission-line reverberation mapping[5] or 23000000 M☉ as measured based on velocity dispersion.[6]

Due to its high brightness in both UV and X-rays, and its prominent and clear active galactic nucleus absorption features, it has been an ideal laboratory for studying the AGN warm-absorber outflows with high-resolution spectroscopy. Over the past few decades, there have been many UV and X-ray case studies of the ionized outflows in NGC 3516.[7] NGC 3516 has been a remarkably variable AGN, showing changes in both the intrinsic continuum[8] and the intrinsic absorption by the ionized outflows.[9] In 2014, the broad lines almost disappeared, probably becoming obstructed, and thus the galaxy has been identified as a changing-look AGN, meaning it changed spectra between type 1 and type 2 AGN.[10]

The galaxy has been found to emit radiowaves, with the source extending towards the north for about 0.65 arcseconds.[11] That structure is a bit curved and probably is related to the gaseous outflow.[12] A spiral dust feature measuring 3 arcseconds in diameter is visible north of the nucleus. A blue filamentary feature is visible northeast of the nucleus and another blue feature is visible 1.5 arcseconds southwest of the nucleus.[13]

Nearby galaxies

NGC 3516 is a relatively isolated galaxy. Near galaxies include NGC 3147 with its group that NGC 3155, UGC 5570, UGC 5686, and UGC 5689, NGC 3183, NGC 3348, and NGC 3364.[14] Garcia identified NGC 3516 as a member of group that also includes the galaxies NGC 3348, and NGC 3364.[15]

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3516. Retrieved 2016-01-18.
  2. ↑ "Revised NGC Data for NGC 3516". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 3516". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Seyfert, Carl K. (January 1943), "Nuclear Emission in Spiral Nebulae", Astrophysical Journal, 97: 28, Bibcode:1943ApJ....97...28S, doi:10.1086/144488.
  5. ↑ Peterson, Bradley M. (2013). "Measuring the Masses of Supermassive Black Holes" (PDF). Space Science Reviews. 183 (1–4): 253. Bibcode:2014SSRv..183..253P. doi:10.1007/s11214-013-9987-4. S2CID 255067404. Archived from the original (PDF) on 2019-07-26. Retrieved 2023-05-27.
  6. ↑ Nelson, Charles H. (2000). "Black Hole Mass, Velocity Dispersion, and the Radio Source in Active Galactic Nuclei". The Astrophysical Journal. 544 (2): L91–L94. arXiv:astro-ph/0009188. Bibcode:2000ApJ...544L..91N. doi:10.1086/317314. S2CID 117449813.
  7. ↑ Mehdipour, Missagh; Kriss, Gerard A.; Brenneman, Laura W.; Costantini, Elisa; Kaastra, Jelle S.; Branduardi-Raymont, Graziella; Di Gesu, Laura; Ebrero, Jacobo; Mao, Junjie (1 January 2022). "Changing-look Event in NGC 3516: Continuum or Obscuration Variability?". The Astrophysical Journal. 925 (1): 84. arXiv:2112.06297. Bibcode:2022ApJ...925...84M. doi:10.3847/1538-4357/ac42ca. hdl:1887/3515508. This article contains quotations from this source, which is available under the Creative Commons Attribution 4.0 Unported (CC BY 4.0) license.
  8. ↑ Ilić, D.; Oknyansky, V.; Popović, L. č.; Tsygankov, S. S.; Belinski, A. A.; Tatarnikov, A. M.; Dodin, A. V.; Shatsky, N. I.; Ikonnikova, N. P.; Rakić, N.; Kovačević, A.; Marčeta-Mandić, S.; Burlak, M. A.; Mishin, E. O.; Metlova, N. V.; Potanin, S. A.; Zheltoukhov, S. G. (June 2020). "A flare in the optical spotted in the changing-look Seyfert NGC 3516". Astronomy & Astrophysics. 638: A13. arXiv:2004.01308. Bibcode:2020A&A...638A..13I. doi:10.1051/0004-6361/202037532. S2CID 214795047.
  9. ↑ Dunn, Jay P.; Parvaresh, Rozhin; Kraemer, S. B.; Crenshaw, D. Michael (23 February 2018). "Evolution of the Outflows in NGC 3516". The Astrophysical Journal. 854 (2): 166. arXiv:1805.04406. Bibcode:2018ApJ...854..166D. doi:10.3847/1538-4357/aaa95d.
  10. ↑ Shapovalova, A I; Popović, L č; Afanasiev, V L; Ilić, D; Kovačević, A; Burenkov, A N; Chavushyan, V H; Marčeta-Mandić, S; Spiridonova, O; Valdes, J R; Bochkarev, N G; Patiño-Álvarez, V; Carrasco, L; Zhdanova, V E (1 June 2019). "Long-term optical spectral monitoring of a changing-look active galactic nucleus NGC 3516 – I. Continuum and broad-line flux variability". Monthly Notices of the Royal Astronomical Society. 485 (4): 4790–4803. arXiv:1902.10845. doi:10.1093/mnras/stz692.
  11. ↑ Nagar, Neil M.; Wilson, Andrew S.; Mulchaey, John S.; Gallimore, Jack F. (February 1999). "Radio Structures of Seyfert Galaxies. VIII. A Distance- and Magnitude-Limited Sample of Early-Type Galaxies". The Astrophysical Journal Supplement Series. 120 (2): 209–245. arXiv:astro-ph/9901236. Bibcode:1999ApJS..120..209N. doi:10.1086/313183.
  12. ↑ Miyaji, Takamitsu; Wilson, Andrew S.; Perez-Fournon, Ismael (January 1992). "The radio source and bipolar nebulosity in the Seyfert galaxy NGC 3516". The Astrophysical Journal. 385: 137. Bibcode:1992ApJ...385..137M. doi:10.1086/170922.
  13. ↑ Regan, Michael W.; Mulchaey, John S. (June 1999). "Using HUBBLE SPACE TELESCOPE Imaging of Nuclear Dust Morphology to Rule Out Bars Fueling Seyfert Nuclei". The Astronomical Journal. 117 (6): 2676–2694. arXiv:astro-ph/9903053. Bibcode:1999AJ....117.2676R. doi:10.1086/300888.
  14. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025.
  15. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN 0365-0138.
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